In this paper, we examine further radiative shocks in the accretion flow by 2D radiation hydrodynamic
simulations, especially focusing on the super-Eddington accreting flow, compare the results with
theoretical structure of the radiative shock by [1]} and [2]}, and discuss the characteristic features of the radiative shock models in relevance
to Ultraluminous X-ray sources (ULXs). In the next section, we present the model equations
of our simulation setup, then numerical schemes, initial and boundary conditions are
mentioned in section 3. In section 4, the results along with astrophysical significance
are discussed then we summarize and discuss in the final section.
